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Table 1

Observed objects and their parameters.

Object RA Dec Class d V LSR L bol T bol M env References
[h m s] [°] [pc] [km s-1] [L] [K] [M]

NGC 1333 I2A 03:28:55.6 +31:14:37.1 LM 0 235 +7.7 35.7 50 5.1 1, 2, 10, 11
NGC 1333 I4A 03:29:10.5 +31:13:30.9 LM 0 235 +7.2 9.1 33 5.6 1, 2, 10, 11
NGC 1333 I4B 03:29:12.0 +31:13:08.1 LM 0 235 +7.4 4.4 28 3.0 1, 2, 10, 11
Ser SMM1 18:29:49.8 +01:15:20.5 LM 0 415 +8.5 99.0 39 52.1 1, 2, 10, 11, 12
L 1489 04:04:43.0 +26:18:57.0 LM I 140 +7.2 3.8 200 0.2 1, 2, 11, 10
NGC 7129 FIRS2 21:43:01.7 +66:03:24.0 IM 1250 9.8 430 40 50 1, 3
W3 IRS5 02:25:40.6 +62:05:51.0 mIRb 2000 38.4 1.7 × 105 370 424 1, 4, 7
NGC 6334 I 17:20:53.3 35:47:00.0 HMC 1700 7.7 2.6 × 105 100 500 1, 4, 8
NGC 6334 I(N) 17:20:55.2 35:45:04.0 mIRq 1700 3.3 1.9 × 103 30 3826 1, 4, 8
AFGL 2591 20:29:24.9 +40:11:19.5 mIRb 3300 5.5 2.2 × 105 325 320 1, 4
S 140 IRS1 22:19:18.2 +63:18:46.9 mIRb 910 7.1 1.0 × 104 85 100 1, 5, 6
NGC 7538 IRS1 23:13:45.3 +61:28:10.0 UCHII 2800 56.2 1.3 × 105 40 433 1, 4, 9

Notes. Reference position chosen in J2000, distance d, systemic velocity VLSR in the Local Standard of Rest, bolometric luminosity Lbol, bolometric temperature Tbol, and envelope mass Menv. The evolutionary stage is abbreviated for low-mass objects as LM 0 and LM I for Class 0 and I. IM stands for intermediate mass objects. High-mass objects are classified according to van der Tak et al. (2013), based on the scheme presented by Molinari et al. (2008): mIRq for mid-infrared quiet high-mass protostellar object (HMPO), mIRb for mid-infrared bright HMPO, HMC for hot molecular cores, and UCHII for objects reported to contain an ultra-compact HII region.

Reference. (1) van Dishoeck et al. (2011), confusion between NGC 6334 I and I(N) corrected; (2) Kristensen et al. (2012) and references therein; (3) Crimier et al. (2010); (4) van der Tak et al. (2013); (5) Harvey et al. (2012); (6) Dedes et al. (2010); (7) van der Tak et al. (2005); (8) Sandell (2000); (9) Sandell & Sievers (2004); (10) San José-García et al. (2013); (11) Yıldız et al. (2013); (12) Dzib et al. (2010).

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